Deep15 Poster

! ! ! ! A dusty, normal galaxy in the epoch of reionizaon Darach Watson*, Lise Christensen*, Kirsten Knudsen†, Johan Richard‡, Anna Gallazzi*,§, and Michał Michałowski** *Dark Cosmology Centre, U. Copenhagen,†Chalmers University, ‡CRAL Lyon, §INAF-Osservatorio di Arcetri, **IfA, Edinburgh We have detected thermal dust emission from an archetypal early universe star-forming galaxy, A1689-zD1. We detect its stellar continuum in spectroscopy and determine its redshift to be z = 7.5±0.2 from a spectroscopic detection of the Ly" break. A1689-zD1 is a sub-L* galaxy and more representative of the star-forming population during reionisation than other high redshift dusty galaxies found before, with a total star-formation –1 rate of about 12 M⊙ yr . The galaxy is highly evolved: it has a large stellar mass, and is heavily enriched in dust, with a dust-to-gas ratio close to that of the Milky Way. Candidates for the modest galaxies that formed most of the stars in the early universe, at The gravitationally lensing galaxy cluster Abell 1689. The colour image is redshifts z > 7, have been found in large composed with Hubble filters: F105W (blue), F125W (green), F160W (red). The zoomed box (4˝×4˝) shows A1689-zD1. Contours indicate FIR dust emission numbers with extremely deep restframe-UV detected by ALMA at 3, 4, and 5σ local RMS (yellow, positive; white, negative). imaging. But it has proved difficult for existing The ALMA beam (1.36˝#1.15˝) is shown, boom le. Images and noise maps were primary-beam corrected before making the signal-to-noise rao (SNR) maps. Slit spectrographs to characterise them in the UV. posions for the ﬁrst set of X-shooter spectroscopy are overlaid in magenta (dashed The detailed properties of these galaxies could boxes indicate the dither), while the parallacc angle was used in the remaining be measured from dust and cool gas emission at observaons (pink dashed lines). far-infrared wavelengths if the galaxies have become sufficiently enriched in dust and metals. So far, however, the most distant UV-selected galaxy detected in dust emission was only at z = 3.2, and recent results had cast doubt on A1689-zD1 was observed by ALMA at Far-infrared emission requires the whether dust and molecules could be found in 226GHz and is detected at 5.0σ with an production of metals, whether in the typical galaxies at this early epoch. observed flux of 0.61 ± 0.12 mJy in the solid phase as dust, or as ionised combined image gas; to be detected, such galaxies must have enriched their interstellar media with metals and dust. While combinedcombined 319-1 319-2 261261 the metals are primarily produced and distributed via supernova explosions and so metal enrichment happens concurrently with massive star formation, the site of dust production is less certain. However, the mechanism must be very rapid13 and these observations of A1689- zD1 place the strongest direct constraints so far on the rapidity of ALMA signal-to-noise rao (SNR) maps of A1689-zD1. Contours are SNR = 5, 4, 3, 2 (black, solid), –3, –2 (white, dashed). Images and noise maps were primary-beam dust enrichment, occurring within corrected before making SNR maps. Beam sizes are shown, boom le in each panel. Panels are 8˝×8˝. The panels show, le to right, the combined data, the two tunings of observaon 2011.0.00319.S and observaon 2012.1.00261.S. A1689-zD1 is detected, le to right, at 5.0σ, 2.4σ, 3.1σ, and 3.0σ. Natural weighng was used only 500 Myr of the beginning of star- and the visibilies were tapered with a 1˝ circular Gaussian kernel, resulng in beams of 1.36˝×1.15˝, 1.19˝×1.09˝, 1.43˝×1.12˝, 1.43˝×1.17˝ le to right. formation in the universe. The galaxy continuum is detected and can be seen in the binned spectrum (left). The Lyα cutoff is at 1035±24 nm and defines the redshift, z = 7.5±0.2. No lines are detected: EW<4Å for both Lyα and CIII] 1909Å. Our search space is largely free of sky emission lines; they cover only 16% of the range for Lyα, less for CIII]. Fits to the galaxy’s spectral energy distribution yield a lensing- corrected stellar mass of log(M⋆/M⊙) = 9.23, with a light-weighted stellar age, t, of log(t/yr) = 7.91. The lensing-corrected UV 10 luminosity is ~1.8×10 L⊙, resulting in a SFRUV of –1 2.7±0.3 M⊙ yr uncorrected for dust extinction. Spectrum of A1689-zD1. The 1D (lower) and 2D (upper) binned spectra are shown, with the 68% confidence uncertainty on the 1D spectrum in the bottom panel. The redshift z = 7.5 is determined from the Lyα break at 1035 nm. Sky absorption (grey bands) and the best-fit SED (blue line) are shown. The Lyα break is close to the spectrograph’s NIR/VIS arm split, however, the break is clearly detected in the NIR arm alone. A nearby galaxy (z ~ 2) visible in the bottom part of the 2D spectrum is detected in both the VIS and NIR arms. Link to the paper Watson et al. 2015 Nature Background: Abell1689 galaxy cluster doi:10.1038/nature14164.

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